FERMI LARGE AREA TELESCOPE AND MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING ACTIVITY OF PKS 1510-089 BETWEEN 2008 SEPTEMBER AND 2009 JUNE
FERMI LARGE AREA TELESCOPE AND MULTI-WAVELENGTH OBSERVATIONS OF THE FLARING ACTIVITY OF PKS 1510-089 BETWEEN 2008 SEPTEMBER AND 2009 JUNE
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DOI：
10.1088/0004-637x/721/2/1425
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发表时间：
2010-10
期刊：
影响因子：
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通讯作者：
A. Abdo;M. Ackermann;I. Agudo;M. Ajello;A. Allafort;H. Aller;M. Aller;E. Antolini;A. Arkharov;M. Axelsson;U. Bach;L. Baldini;J. Ballet;G. Barbiellini;D. Bastieri;K. Bechtol;R. Bellazzini;A. Berdyugin;B. Berenji;R. Blandford;D. Blinov;E. Bloom;M. Boettcher;E. Bonamente;A. Borgland;A. Bouvier;J. Bregeon;A. Brez;M. Brigida;P. Bruel;R. Buehler;C. Buemi;T. Burnett;S. Buson;G. Caliandro;R. Cameron;P. Caraveo;D. Carosati;S. Carrigan;J. Casandjian;E. Cavazzuti;C. Cecchi;O. Celik;A. Chekhtman;Wen-Ping Chen;C. C. Cheung-C.;J. Chiang;S. Ciprini;R. Claus;J. Cohen-Tanugi;J. Conrad;S. Corbel;L. Costamante;C. Dermer;A. Angelis;F. Palma;D. Donato;E. Silva;P. Drell;R. Dubois;D. Dumora;C. Farnier;C. Favuzzi;S. Fegan;E. Ferrara;W. Focke;E. Forne;P. Fortin;Y. Fukazawa;S. Funk;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;S. Germani;B. Giebels;N. Giglietto;F. Giordano;M. Giroletti;T. Glanzman;G. Godfrey;I. Grenier;J. Grove;S. Guiriec;M. Gurwell;C. Gusbar;J. Gómez;D. Hadasch;V. Hagen-Thorn;M. Hayashida;E. Hays;D. Horan;R. Hughes;G. Jóhannesson;A. Johnson;W. Johnson;T. Kamae;H. Katagiri;J. Kataoka;N. Kawai;G. Kimeridze;J. Knödlseder;T. Konstantinova;E. Kopatskaya;E. Koptelova;Y. Kovalev;O. Kurtanidze;M. Kuss;A. Lähteenmäki;J. Lande;V. Larionov;E. Larionova;L. Larionova;S. Larsson;L. Latronico;S. Lee;P. Leto;M. Lister;F. Longo;F. Loparco;B. Lott;M. Lovellette;P. Lubrano;G. Madejski;A. Makeev;E. Massaro;M. Mazziotta;W. Mcconville;J. Mcenery;I. McHardy;P. Michelson;W. Mitthumsiri;T. Mizuno;A. Moiseev;C. Monte;M. Monzani;D. Morozova;A. Morselli;I. Moskalenko;S. Murgia;M. Naumann-Godo;M. Nikolashvili;P. Nolan;J. Norris;E. Nuss;M. Ohno;T. Ohsugi;A. Okumura;N. Omodei;E. Orlando;J. Ormes;M. Ozaki;D. Paneque;J. Panetta;D. Parent;M. Pasanen;V. Pelassa;M. Pepe;M. Pesce-Rollins;F. Piron;T. Porter;A. Pushkarev;S. Rainò;C. Raiteri;R. Rando;M. Razzano;A. Reimer;O. Reimer;R. Reinthal;J. Ripken;S. Ritz;M. Roca-Sogorb;A. Rodríguez;M. Roth;P. Roustazadeh;F. Ryde;H. Sadrozinski;A. Sander;J. Scargle;C. Sgro’;L. Sigua;P. Smith;K. Sokolovsky;G. Spandre;P. Spinelli;Jean-Luc Starck;M. Strickman;D. Suson;H. Takahashi;Tadayuki Takahashi;L. Takalo;Takaaki Tanaka;B. Taylor;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;M. Tornikoski;D. Torres;G. Tosti;A. Tramacere;C. Trigilio;I. Troitsky;G. Umana;T. Usher;J. Vandenbroucke;V. Vasileiou;N. Vilchez;M. Villata;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;Z. Yang;T. Ylinen;M. Ziegler
中科院分区：
文献类型：
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作者：
A. Abdo;M. Ackermann;I. Agudo;M. Ajello;A. Allafort;H. Aller;M. Aller;E. Antolini;A. Arkharov;M. Axelsson;U. Bach;L. Baldini;J. Ballet;G. Barbiellini;D. Bastieri;K. Bechtol;R. Bellazzini;A. Berdyugin;B. Berenji;R. Blandford;D. Blinov;E. Bloom;M. Boettcher;E. Bonamente;A. Borgland;A. Bouvier;J. Bregeon;A. Brez;M. Brigida;P. Bruel;R. Buehler;C. Buemi;T. Burnett;S. Buson;G. Caliandro;R. Cameron;P. Caraveo;D. Carosati;S. Carrigan;J. Casandjian;E. Cavazzuti;C. Cecchi;O. Celik;A. Chekhtman;Wen-Ping Chen;C. C. Cheung-C.;J. Chiang;S. Ciprini;R. Claus;J. Cohen-Tanugi;J. Conrad;S. Corbel;L. Costamante;C. Dermer;A. Angelis;F. Palma;D. Donato;E. Silva;P. Drell;R. Dubois;D. Dumora;C. Farnier;C. Favuzzi;S. Fegan;E. Ferrara;W. Focke;E. Forne;P. Fortin;Y. Fukazawa;S. Funk;P. Fusco;F. Gargano;D. Gasparrini;N. Gehrels;S. Germani;B. Giebels;N. Giglietto;F. Giordano;M. Giroletti;T. Glanzman;G. Godfrey;I. Grenier;J. Grove;S. Guiriec;M. Gurwell;C. Gusbar;J. Gómez;D. Hadasch;V. Hagen-Thorn;M. Hayashida;E. Hays;D. Horan;R. Hughes;G. Jóhannesson;A. Johnson;W. Johnson;T. Kamae;H. Katagiri;J. Kataoka;N. Kawai;G. Kimeridze;J. Knödlseder;T. Konstantinova;E. Kopatskaya;E. Koptelova;Y. Kovalev;O. Kurtanidze;M. Kuss;A. Lähteenmäki;J. Lande;V. Larionov;E. Larionova;L. Larionova;S. Larsson;L. Latronico;S. Lee;P. Leto;M. Lister;F. Longo;F. Loparco;B. Lott;M. Lovellette;P. Lubrano;G. Madejski;A. Makeev;E. Massaro;M. Mazziotta;W. Mcconville;J. Mcenery;I. McHardy;P. Michelson;W. Mitthumsiri;T. Mizuno;A. Moiseev;C. Monte;M. Monzani;D. Morozova;A. Morselli;I. Moskalenko;S. Murgia;M. Naumann-Godo;M. Nikolashvili;P. Nolan;J. Norris;E. Nuss;M. Ohno;T. Ohsugi;A. Okumura;N. Omodei;E. Orlando;J. Ormes;M. Ozaki;D. Paneque;J. Panetta;D. Parent;M. Pasanen;V. Pelassa;M. Pepe;M. Pesce-Rollins;F. Piron;T. Porter;A. Pushkarev;S. Rainò;C. Raiteri;R. Rando;M. Razzano;A. Reimer;O. Reimer;R. Reinthal;J. Ripken;S. Ritz;M. Roca-Sogorb;A. Rodríguez;M. Roth;P. Roustazadeh;F. Ryde;H. Sadrozinski;A. Sander;J. Scargle;C. Sgro’;L. Sigua;P. Smith;K. Sokolovsky;G. Spandre;P. Spinelli;Jean-Luc Starck;M. Strickman;D. Suson;H. Takahashi;Tadayuki Takahashi;L. Takalo;Takaaki Tanaka;B. Taylor;J. Thayer;J. Thayer;D. Thompson;L. Tibaldo;M. Tornikoski;D. Torres;G. Tosti;A. Tramacere;C. Trigilio;I. Troitsky;G. Umana;T. Usher;J. Vandenbroucke;V. Vasileiou;N. Vilchez;M. Villata;V. Vitale;A. Waite;Pengfei Wang;B. Winer;K. Wood;Z. Yang;T. Ylinen;M. Ziegler
本文报道了PKS 1510-089 （z = 0.361的平谱射电类星体）在2008年9月至2009年6月的高活跃期的多波长观测结果。在这11个月期间，该源在光学、紫外和γ射线波段具有复杂的变化特征，时间尺度低至6-12小时。2009年3月26日记录到的最亮γ射线各向同性亮度为2 × 1048 erg s−1。费米大面积望远镜能量范围内的光谱显示出一个温和的曲率，可以很好地描述为对数抛物线定律，并且可以理解为由于Klein-Nishina效应。γ射线通量与其他波长具有复杂的相关性。与x射线波段没有相关性，与紫外波段有弱相关性，与光通量有显著相关性。γ射线通量似乎比光学通量领先大约13天。通过紫外光度测量，我们估计黑洞质量为5.4 × 108 M☉，吸积率为0.5 M☉yr - 1。尽管与非常明亮和遥远的FSRQs相比，PKS 1510-089的热和非热输出功率较小，但它表现出相当大的康普顿优势和在最强大的γ射线类星体中观察到的显著的蓝色凸起（BBB）。在2009年5月的历史最大光学状态下，BBB仍然很突出，但光学/紫外光谱指数比静止状态更弱。这似乎表明，在最高光态时，BBB并不完全由同步辐射主导。我们假设一个轻子场景来模拟宽带频谱，其中逆康普顿发射主要是由外部产生的软光子散射到射流中。由此得出的依赖于模型的射流能量含量与射流由吸积盘提供动力的情况相兼容，其总效率在克尔黑洞极限内。
We report on the multi-wavelength observations of PKS 1510-089 (a flat spectrum radio quasar (FSRQ) at z = 0.361) during its high activity period between 2008 September and 2009 June. During this 11 month period, the source was characterized by a complex variability at optical, UV, and γ-ray bands, on timescales down to 6–12 hr. The brightest γ-ray isotropic luminosity, recorded on 2009 March 26, was ≃2 × 1048 erg s−1. The spectrum in the Fermi Large Area Telescope energy range shows a mild curvature described well by a log-parabolic law, and can be understood as due to the Klein–Nishina effect. The γ-ray flux has a complex correlation with the other wavelengths. There is no correlation at all with the X-ray band, a weak correlation with the UV, and a significant correlation with the optical flux. The γ-ray flux seems to lead the optical one by about 13 days. From the UV photometry, we estimated a black hole mass of ≃5.4 × 108 M☉ and an accretion rate of ≃0.5 M☉ yr−1. Although the power in the thermal and non-thermal outputs is smaller compared to the very luminous and distant FSRQs, PKS 1510-089 exhibits a quite large Compton dominance and a prominent big blue bump (BBB) as observed in the most powerful γ-ray quasars. The BBB was still prominent during the historical maximum optical state in 2009 May, but the optical/UV spectral index was softer than in the quiescent state. This seems to indicate that the BBB was not completely dominated by the synchrotron emission during the highest optical state. We model the broadband spectrum assuming a leptonic scenario in which the inverse Compton emission is dominated by the scattering of soft photons produced externally to the jet. The resulting model-dependent jet energetic content is compatible with a scenario in which the jet is powered by the accretion disk, with a total efficiency within the Kerr black hole limit.